Use the following formula (fitted to data) L Mo/year gR M = -4x10-13n for the mass loss of asymptotic giant branch stars to: a) explain why L, g (gravity on surface), and R enter the equation the way they do (nominator or denominator). b) show that the expression for M is equivalent to LR M = -4x10-137 Mo/year - M c) estimate the mass loss rate of a star with M = 1 Mo, L = 7000 Lo,T = 3000 K. Assume n = 1 and use the Stefan-Boltzmann equation to calculate R (in Ro). %3D

Use the following formula (fitted to data) L Mo/year gR M = -4x10-13n for the mass loss of asymptotic giant branch stars to: a) explain why L, g (gravity on surface), and R enter the equation the way they do (nominator or denominator). b) show that the expression for M is equivalent to LR M = -4x10-137 Mo/year - M c) estimate the mass loss rate of a star with M = 1 Mo, L = 7000 Lo,T = 3000 K. Assume n = 1 and use the Stefan-Boltzmann equation to calculate R (in Ro). %3D

College Physics

11th Edition

ISBN:9781305952300

Author:Raymond A. Serway, Chris Vuille

Publisher:Raymond A. Serway, Chris Vuille

Chapter1: Units, Trigonometry. And Vectors

Section: Chapter Questions

Problem 1CQ: Estimate the order of magnitude of the length, in meters, of each of the following; (a) a mouse, (b)...

See similar textbooks

Similar questions

Can you please help with Part 3 of 3?
Cluster Sizes. An open cluster is a collection of 10 to 1000 stars in a region about 25 pc in diameter. About how far apart are the stars in an open cluster in units of pc? (Hints: What share of the cluster's volume belongs to a single 4 Tr. Use the cited value for the maximum number of stars in your calculation.) star? The volume of a sphere is pc.
A supernova’s energy is often compared to the total energy output of the Sun over its lifetime. Using the Sun’s current luminosity, calculate the total solar energy output, assuming a 1010 year main-sequence lifetime. Using Einstein’s formula E=mc2 calculate the equivalent amount of mass, expressed in Earth masses. [Hint: The total energy output of the Sun over its lifetime is given by its current luminosity times the number of seconds in a year times its ten billion-year lifetime; ; mass of earth = 6×1024kg; c = 3×108m/s. Your answer should be 200-300 Earth masses.]
if a star is converted every bit of its mass. into energy the conversion efficiency would be 100%. however no star is this efficient in its energy production stars with less than 1.3 solar masses convert hydrogen into helium with an efficiency of only 0.7%. besring in mind that aldebaram has a mass of 2.32*10^30 kg. how long will it live if it converts all of its hydrogen into helium with an efficiency of 0.7%. 1 year = 365.25 days. lifetime= years
A) A typical dust grain has a radius of about 0.1 micrometers and a mass of 10-14 grams. Roughly how many dust particles are in a cloud containing 1000 Msun of dusty gas if 1% of the cloud's mass is in the form of dust grains? B) What surface area would be covered by these grains if you put them side by side? Assume these grains are spherical. Answer in square light-years. C) Estimate the total surface area covered by the cloud assuming it's matter density is like that of a typical molecular cloud, about 10-21 g/cm3 (Hint: first calculate the clouds volume from it's mass and density, then determine its radius using the formula for volume of a sphere) Answer in square light-years. D) Comparing all above answers, What are the chances (very roughly) that a photon passing through the cloud will hit a dust grain?
If interstellar dust makes an RR Lyrae variable star look 7 magnitudes fainter than the star should, by how much will you over- or underestimate its distance? (Hint: Use the magnitude-distance formula d = 10 mv - Mv + 5)/5.) destimate dactual = Is your calculated value an over- or underestimate? O overestimate O underestimate
Calculate the angular diameter of a prestellar nebula of radius 125 AU lying 150 pc from Earth. angular diameter = 15. ΑΣΦ B ? arc seconds
How many years? Thank you!
Explain pre main sequence evolution, early post main sequence evolution and advanced evolutionary stages.
Describe T-Tauri stars and Herbig–Haro objects. In what phase do they occur in the lifespan of a star?
Pls help ASAP. Pls show all work.
What the main differences that can occur between the life cycles of a Sun-sized star and a massive star? Plz help me asap with good type anwers in 3-4 sentences plzz